2006
DOI: 10.1111/j.1365-2966.2006.10946.x
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INTEGRAL and XMM-Newton observations of LSI +61  303

Abstract: LSI +61° 303 is one of the few X‐ray binaries with Be star companion from which both radio and high‐energy γ‐ray emission have been observed. We present XMM–Newton and INTEGRAL observations which reveal variability of the X‐ray spectral index of the system. The X‐ray spectrum is hard (photon index Γ≃ 1.5) during the orbital phases of both high and low X‐ray flux. However, the spectrum softens at the moment of transition from high to low X‐ray state. The spectrum of the system in the hard X‐ray band does not re… Show more

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Cited by 83 publications
(125 citation statements)
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“…Recently the orbital modulation was seen by the MAGIC Cherenkov air-showers telescope in ultra high energy gamma rays (above 400 GeV), clinching the case for the identification of LS I +61 • 303 as a gamma-ray emitter (Albert et al 2006). This was also confirmed in the hard X-ray energies (up to 100 keV) by INTEGRAL observation of variable emission, peaking at phase ∼0.55 of the orbital modulation (Chernyakova et al 2006;Hermsen & Kuiper 2007).…”
Section: Ls I +61mentioning
confidence: 54%
See 1 more Smart Citation
“…Recently the orbital modulation was seen by the MAGIC Cherenkov air-showers telescope in ultra high energy gamma rays (above 400 GeV), clinching the case for the identification of LS I +61 • 303 as a gamma-ray emitter (Albert et al 2006). This was also confirmed in the hard X-ray energies (up to 100 keV) by INTEGRAL observation of variable emission, peaking at phase ∼0.55 of the orbital modulation (Chernyakova et al 2006;Hermsen & Kuiper 2007).…”
Section: Ls I +61mentioning
confidence: 54%
“…Although in soft X-rays there were no doubts from the start about the source identification , the X-ray observations, aimed at studying the orbital modulation, proceeded in parallel with the gamma-ray ones, using all the X-ray instruments active over the past 30 years: Einstein , ROSAT (Goldoni & Mereghetti 1995;Taylor et al 1996), ASCA (Leahy et al 1997), RossiXTE (Paredes et al 1997;Harrison et al 2000;Greiner & Rau 2001;Leahy 2001;Grundstrom et al 2007), INTEGRAL (Chernyakova et al 2006;Hermsen & Kuiper 2007), BeppoSAX, XMM-Newton (Sidoli et al 2006), and Chandra (Paredes et al 2007).…”
Section: Ls I +61mentioning
confidence: 99%
“…The shape of the combined spectrum suggests that if the low and high-energy emissions are related, the peak energy should be between 1-100 MeV. A similar spectrum is observed in LS I+61 • 303; (Chernyakova et al 2009), though it could be modelled under the assumption of a pulsar-powered source. Because we know nothing on the nature of the source, it is not possible to use physical models at this stage.…”
Section: The Combined X-ray and Gamma Ray Spectrummentioning
confidence: 86%
“…This source, also shown in Fig. 1, is found at 5.22 from 1FGL J1227.9-4852 and at 4.12 from the XSS J1227 optical 2 The broad-band 0.2-100 keV fluxes of LS I+61 • 303, LS 5039 and Cyg X-3 are taken from Chernyakova et al (2009), Takahashi et al (2009 and Hjalmarsdotter et al (2009), respectively. 3 http://www.heasarc.gsfc.nasa.gov/W3Browse/all/radio.…”
Section: Discussionmentioning
confidence: 99%
“…If θ flow = 0 then intrinsic emission in the co-moving frame is boosted in the observer frame at inferior conjunction and deboosted at superior conjunction. (Chernyakova et al 2006(Chernyakova et al , 2009Acciari et al 2009;Anderhub et al 2009). The application to these gamma-ray binaries is discussed in Sect.…”
Section: Introductionmentioning
confidence: 99%